This star was first catalogued by American astronomer Frank Elmore Ross in 1925. Ross 154 was found to be a UV Ceti-type flare star, with a mean time between major flares of about two days.[1] The first such flare activity was observed from Australia in 1951 when the star increased in magnitude by 0.4. Usually, the star will increase by 3–4 magnitudes during a flare.

Ross 154 is an X-ray source and it has been detected by several X-ray observatories. The quiescent X-ray luminosity is about 9 × 1027 ergs s−1. X-ray flare emission from this star has been observed by Chandra observatory, with a particularly large flare emitting 2.3 × 1033 erg.[3]

This is a red dwarf star that is generating energy through the nuclear fusion of hydrogen at its core. It has an estimated 17% of the Sun's mass and 24% of the Sun's radius, but it is radiating only 0.38% of the luminosity of the Sun. This is probably a young star with an age of less than a billion years.<warg/> The abundance of elements heavier than helium is about half that in the Sun.